Table 2
Hα radii for the IFS sample of U/LIRGs observed with VIMOS and INTEGRAL.
| IRAS ID | Other ID | Subsample | r1/2-Hα (A/2) | r1/2-Hα (CoG) | Comment |
| name | (kpc) | (kpc) | |||
| (1) | (2) | (3) | (4) | (5) | (6) |
|
|
|||||
| VIMOS | |||||
|
|
|||||
| F01159−4443N | ESO−244−G012 | N | 0.35 ± 0.10 | 0.36 ± 0.11 | 1, 2 |
| F01341−3735N | ESO−297−G011 | N | >1.36 ± 0.41 | >1.89 ± 0.57 | 2, 3 |
| F01341−3735S | ESO−297−G012 | N | 0.23 ± 0.11 | 0.22 ± 0.11 | 1 |
| F04315−0840 | NGC 1614 | N | 0.51 ± 0.15 | 0.51 ± 0.15 | |
| F05189−2524 | Y | <0.28 | <0.28 | 0, 5, 6 | |
| F06035−7102 | Y | 3.72 ± 1.12 | 7.06 ± 2.12 | ||
| F06076−2139N | N | <0.25 | <0.25 | 0 | |
| F06076−2139S | N | 0.48 ± 0.24 | 0.45 ± 0.22 | 1, 7 | |
| F06206−6315 | Y | 2.53 ± 0.76 | 4.43 ± 1.33 | 5 | |
| F06259−4708N | N | 0.71 ± 0.21 | 0.74 ± 0.22 | 9 | |
| F06259−4708C | Y | 1.16 ± 0.35 | 1.31 ± 0.39 | 8 | |
| F06259−4708S | Y | 1.45 ± 0.44 | 1.93 ± 0.58 | 8 | |
| F06295−1735 | ESO−557−G002 | N | 1.91 ± 0.57 | 2.46 ± 0.74 | 2 |
| F06592−6313 | N | 0.35 ± 0.17 | 0.39 ± 0.20 | 1 | |
| F07027−6011N | AM 0702−601 | N | 0.47 ± 0.24 | 0.50 ± 0.25 | 1, 5, 6, 10 |
| F07027−6011S | Y | 0.63 ± 0.19 | 0.63 ± 0.19 | ||
| F07160−6215 | NGC 2369 | N | >0.54 ± 0.16 | >0.86 ± 0.26 | 3 |
| 08355−4944 | N | 0.59 ± 0.18 | 0.64 ± 0.19 | 2 | |
| F08520−6850 | ESO60−IG016 | Y | 1.02 ± 0.31 | 1.04 ± 0.31 | 2 |
| 09022−3615 | Y | 1.30 ± 0.39 | 1.20 ± 0.36 | ||
| F09437+0317N | IC-563 | N | >2.20 ± 0.66 | >3.22 ± 0.97 | 3 |
| F09437 + 0317S | IC-564 | N | >1.93 ± 0.58 | >3.08 ± 0.92 | 3 |
| F10015−0614 | NGC-3110 | N | >1.95 ± 0.59 | >2.66 ± 0.80 | 3 |
| F10038−3338 | IC2545 | Y | 0.51 ± 0.26 | 0.69 ± 0.23 | 1 |
| F10257−4339 | NGC 3256 | N | >1.01 ± 0.30 | >1.37 ± 0.41 | 3 |
| F10409−4556 | ESO−264−G036 | N | >1.78 ± 0.53 | >3.24 ± 0.97 | 3 |
| F10567−4310 | ESO−264−G057 | N | >1.61 ± 0.48 | >3.69 ± 1.11 | 2, 3 |
| F11255−4120 | ESO−319−G022 | N | 1.25 ± 0.38 | 2.70 ± 0.81 | |
| F11506−3851 | ESO−320−G030 | N | 0.68 ± 0.21 | 1.05 ± 0.31 | |
| F12043−3140N | ESO−440−IG 058 | N | 0.24 ± 0.12 | 0.18 ± 0.09 | 1, 7 |
| F12043−3140S | ESO−440−IG 058 | N | >1.38 ± 0.41 | >2.92 ± 0.88 | 3 |
| F12115−4656 | ESO−267−G030 | N | 1.34 ± 0.40 | 1.55 ± 0.46 | |
| 12116−5615 | N | 0.28 ± 0.14 | 0.29 ± 0.14 | 1 | |
| F13001−2339 | ESO−507−G070 | N | 0.88 ± 0.26 | 0.91 ± 0.27 | |
| F13229−2934 | NGC 5135 | N | >0.52 ± 0.16 | >0.53 ± 0.16 | 3,5 |
| F14544−4255E | IC 4518 | N | >0.94 ± 0.28 | >1.06 ± 0.32 | 3 |
| F14544−4255W | IC 4518 | N | 0.57 ± 0.17 | 0.66 ± 0.20 | 5 |
| F17138−1017 | N | 0.56 ± 0.17 | 0.63 ± 0.19 | ||
| F18093−5744N | N | 1.10 ± 0.33 | 1.56 ± 0.47 | ||
| F18093−5744C | N | 0.35 ± 0.11 | 0.34 ± 0.10 | 6 | |
| F18093−5744S | N | 0.84 ± 0.25 | 1.21 ± 0.36 | 7 | |
| F21130−4446 | Y | 1.59 ± 0.48 | 1.89 ± 0.57 | 2 | |
| F21453−3511 | NGC 7130 | N | >1.04 ± 0.31 | >2.27 ± 0.68 | 3, 5, 6 |
| F22132−3705 | IC 5179 | N | >1.56 ± 0.47 | >1.90 ± 0.57 | 3 |
| F22491−1808 | N | 1.70 ± 0.50 | 2.30 ± 0.70 | ||
| F23128−5919 | AM 2312−591 | Y | 2.01 ± 0.60 | 3.01 ± 0.90 | 5, 6 |
|
|
|||||
| INTEGRAL | |||||
|
|
|||||
| 06268+3509 | Y | 3.74 ± 1.50 | 4.33 ± 1.73 | ||
| 06487+2208 | Y | 0.98 ± 0.49 | 1.12 ± 0.56 | 1, 4 | |
| F08572+3515 | Y | 1.85 ± 0.74 | 2.70 ± 1.08 | ||
| F11087+5351 | Y | 2.49 ± 1.00 | 3.76 ± 1.50 | 4, 6 | |
| Arp299E / IC694a | N | > 0.68 ± 0.27 | > 1.03 ± 0.41 | 3 | |
| F11257+5850a | Arp299W /NGC3690a | N | > 0.53 ± 0.21 | > 0.67 ± 0.27 | 3,5 |
| F12112+0305 | Y | 2.60 ± 1.04 | 3.48 ± 1.39 | ||
| F12490−1009 | N | 1.77 ± 0.71 | 1.58 ± 0.63 | ||
| F13156+0435N | Y | 1.96 ± 0.78 | 1.99 ± 0.80 | ||
| F13156+0435S | Y | 2.66 ± 1.06 | 2.68 ± 1.07 | ||
| F13428+5608 | Mrk 273 | N | 1.29 ± 0.52 | 1.71 ± 0.68 | 5 |
| F13536+1836 | Mrk 463 | Y | <0.44 | <0.44 | 0, 5, 6 |
| F14060+2919 | Y | 1.30 ± 0.65 | 1.13 ± 0.57 | 1 | |
| F14348−1447 | Y | 3.82 ± 1.53 | 4.68 ± 1.87 | ||
| F15206+3342 | Y | <1.00 | <1.00 | 0 | |
| F15250+3609 | Y | <0.48 | <0.48 | 0 | |
| F15327+2340 | Arp 220 | N | 0.63 ± 0.25 | 0.61 ± 0.24 | |
| F16007+3743 | Y | 3.67 ± 1.47 | 6.15 ± 2.46 | ||
| F17207−0014 | Y | 0.90 ± 0.36 | 1.01 ± 0.40 | ||
| F18580+6527 | Y | 2.37 ± 0.95 | 2.09 ± 0.84 | 5 | |
Notes. Columns: (1) and (2) identification; (3) indicates whether or not the object is in the subsample of U/LIRGs with L(Hα) and spatial resolution similar to those of high-z samples (see text); (4) Hα radius obtained with the A/2 method; (5) Hα radius obtained with the Curve-of-Growth method; (6) comments with the following code: 0:Hα half-light radius equal or smaller than the PSF (i.e. unresolved), 1: Hα half-light radius smaller than 1.25 times the radius of the PSF and therefore, with larger uncertainty, 2: Noisy continuum, 3: Limited FoV, 4: Observed with INTEGRAL/SB1 configuration, 5: evidence for an AGN according to the emission line ratios (see GM09, and compilation of RZ11), 6: evidence for a broad line associated to Hα suggesting the presence of an AGN. 7: the Lir for this object is unknown, and therefore it is not included in the analysis. 8: for this object the individual Lir is not known, but taking into account that the whole system has Lir = 11.91, and (reddening corrected) Hα luminosities above 1042 erg s-1 it is likely a LIRG, and it kept for the analysis. 9: for this object the individual Lir is not accurate known, but taking into account that the whole system has Lir = 11.91 and according to Spitzer MIPS (24 μm) data it carries a large fraction of the IR flux, it is likely a LIRG. 10: this object likely to have a strong AGN contamination so it was not included in the sample for comparison with high-z samples (see text). The values reported for the CoG and A/2 methods have been deconvolved in quadrature from the radii associated to stars. We used an averaged value of r1/2 (PSF) = 1.07 arcsec for VIMOS data from 7 stars located within the FoV of the science pointings. For the INTEGRAL-SB2 data, that value was scaled according to the spaxel scale, and for SB1 (which was used on average under better seeing conditions) we adopted 0.9 arcsec, as inferred from the Mrk 231 observations. Typical errors are estimated to be 30 percent, except for cases with comments 1 and 2 for which are increased to 50 percent. Values limited by FoV (comment 3) should be considered as lower limits. For radii derived from the INTEGRAL data, typical errors are estimated to be somewhat larger (40 percent), since no direct measurements for the PSF were available. Further details on these galaxies can be found in GM06 (INTEGRAL data) and RZ11 (VIMOS data).
Identification as in García-Marín et al. (2006).
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